ULTRA HIGH ENERGY NEUTRINO TELESCOPES

2006 ◽  
Vol 21 (08n09) ◽  
pp. 1914-1924
Author(s):  
PER OLOF HULTH
Keyword(s):  
Lake Baikal ◽  
High Energy ◽  
Atmospheric Neutrinos ◽  
South Pole ◽  
Ultra High Energy ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Neutrino Astronomy

The Neutrino Telescopes NT-200 in Lake Baikal, Russia and AMANDA at the South Pole, Antarctica have now opened the field of High Energy Neutrino Astronomy. Several other Neutrino telescopes are in the process of being constructed or very near realization. Several thousands of atmospheric neutrinos have been observed with energies up to several 100 TeV but so far no evidence for extraterrestrial neutrinos has been found.

scholarly journals Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

2012 ◽  
Vol 85 (6) ◽  
Author(s):  
I. Kravchenko ◽  
S. Hussain ◽  
D. Seckel ◽  
D. Besson ◽  
E. Fensholt ◽  
...  
Keyword(s):  
High Energy ◽  
South Pole ◽  
Ultra High Energy ◽  
Future Prospects ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Detection ◽  
Energy Neutrino

EARLY YEARS OF HIGH-ENERGY NEUTRINO PHYSICS IN COSMIC RAYS AND NEUTRINO ASTRONOMY (1957-1962)

2006 ◽  
Vol 21 (supp01) ◽  
pp. 1-11 ◽  
Author(s):  
IGOR ZHELEZNYKH
Keyword(s):  
Neutrino Physics ◽  
Large Scale ◽  
High Energy ◽  
Early Years ◽  
Atmospheric Neutrinos ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Deep Underground ◽  
Neutrino Astronomy

Ideas of deep underground and deep underwater detection of high-energy cosmic neutrinos were firstly suggested by Moisey Markov in the end of 50th. Frederic Reines was one of those who first detected high-energy atmospheric neutrinos in underground experiments in the middle of 60th (as well as low energy reactor neutrinos 10 years earlier!). Markov and Reines closely collaborated in 70th – 80th in discussion of alternative techniques for large-scale neutrino telescopes. Some events of 50 – 80 years relating to the development of a new branch of Astronomy – the High-Energy Neutrino Astronomy, in which Markov and Reines took part, were described in my talk at ARENA Workshop. Below the first part of my talk at the Workshop is presented describing discussions and meetings the neutrino physics and astrophysics relating to the period 1957-1962 when I was Markov's student and later post-graduated student.

scholarly journals On the age vs depth and optical clarity of deep ice at the South Pole

1995 ◽  
Vol 41 (139) ◽  
pp. 445-454
Author(s):  
Keyword(s):  
Visible Light ◽  
High Energy ◽  
Dust Concentration ◽  
Cherenkov Light ◽  
South Pole ◽  
The South ◽  
High Energy Neutrino ◽  
Arrival Times ◽  
Energy Neutrino ◽  
Crystal Boundaries

AbstractThe first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800-1000 m in ice at the South Pole, During the 1995-96 season, as many as six more strings will be deployed at greater depths. Provided absorption, scattering and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of Cherenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the interval 1600-2100 m will be suitably transparent for a future 1 km3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 k year BP.

scholarly journals IceCube: A Kilometer-Scale Neutrino Observatory at the South Pole

2005 ◽  
Vol 13 ◽  
pp. 949-950
Author(s):  
Francis Halzen
Keyword(s):  
Cosmic Rays ◽  
Particle Physics ◽  
High Energy ◽  
Neutrino Telescope ◽  
South Pole ◽  
Neutrino Detector ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Diversity Of Science

AbstractSolving the century-old puzzle of how and where cosmic rays are accelerated mostly drives the design of high-energy neutrino telescopes. It calls, along with a diversity of science goals reaching particle physics, astrophysics and cosmology, for the construction of a kilometer-scale neutrino detector. This led to the IceCube concept to transform a kilometer cube of transparent Antarctic Ice, one mile below the South Pole, into a neutrino telescope.

scholarly journals Acoustic parametric techniques for neutrino telescopes

2019 ◽  
Vol 216 ◽  
pp. 04001
Author(s):  
Miguel Ardid ◽  
Dídac D. Tortosa ◽  
Carlos David Llorens Alvarez ◽  
Juan A. Martínez-Mora ◽  
María Saldaña
Keyword(s):  
High Energy ◽  
Neutrino Interaction ◽  
Ultra High Energy ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Acoustic Signature ◽  
Acoustic Sources

In this work, we present a compact transmitter array based on the parametric acoustic sources effect able to reproduce the acoustic signature of an Ultra-High Energy neutrino interaction in water. We also propose to use directive transducers employing the parametric technique for the characterization of piezo-ceramic sensors contained in the KM3NeT Digital Optical Modules. This technique can minimize the need for tests in an anechoic tank.

scholarly journals On the age vs depth and optical clarity of deep ice at the South Pole

1995 ◽  
Vol 41 (139) ◽  
pp. 445-454 ◽  
Author(s):  
Keyword(s):  
Visible Light ◽  
High Energy ◽  
Dust Concentration ◽  
Cherenkov Light ◽  
South Pole ◽  
The South ◽  
High Energy Neutrino ◽  
Arrival Times ◽  
Energy Neutrino ◽  
Crystal Boundaries

AbstractThe first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800-1000 m in ice at the South Pole, During the 1995-96 season, as many as six more strings will be deployed at greater depths. Provided absorption, scattering and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of Cherenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the interval 1600-2100 m will be suitably transparent for a future 1 km3observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 k year BP.

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